scholarly journals The Effect of Mass Segregation on Gravitational Wave Sources near Massive Black Holes

2006 ◽  
Vol 645 (2) ◽  
pp. L133-L136 ◽  
Author(s):  
Clovis Hopman ◽  
Tal Alexander
Keyword(s):  
Black Holes ◽  
Gravitational Wave ◽  
Massive Black Holes ◽  
Mass Segregation

scholarly journals Fake Massive Black Holes in the Milli-Hertz Gravitational-wave Band

2020 ◽  
Vol 896 (2) ◽  
pp. 171
Author(s):  
Xian Chen ◽  
Ze-Yuan Xuan ◽  
Peng Peng
Keyword(s):  
Black Holes ◽  
Gravitational Wave ◽  
Wave Band ◽  
Massive Black Holes

scholarly journals The Clustering Dynamics of Primordial Black Boles in N-Body Simulations

Universe ◽  
2021 ◽  
Vol 7 (1) ◽  
pp. 18
Author(s):  
Manuel Trashorras ◽  
Juan García-Bellido ◽  
Savvas Nesseris
Keyword(s):  
Black Holes ◽  
Binary Systems ◽  
Orbital Parameter ◽  
Galactic Halos ◽  
Massive Black Holes ◽  
Close Encounters ◽  
Mass Ratios ◽  
History Of ◽  
Mass Segregation ◽  
Rate Of Evaporation

We explore the possibility that Dark Matter (DM) may be explained by a nonuniform background of approximately stellar mass clusters of Primordial Black Holes (PBHs) by simulating the evolution from recombination to the present with over 5000 realisations using a Newtonian N-body code. We compute the cluster rate of evaporation and extract the binary and merged sub-populations along with their parent and merger tree histories, lifetimes and formation rates, the dynamical and orbital parameter profiles, the degree of mass segregation and dynamical friction and power spectrum of close encounters. Overall, we find that PBHs can constitute a viable DM candidate, and that their clustering presents a rich phenomenology throughout the history of the Universe. We show that binary systems constitute about 9.5% of all PBHs at present, with mass ratios of q¯B=0.154, and total masses of m¯T,B=303M⊙. Merged PBHs are rare, about 0.0023% of all PBHs at present, with mass ratios of q¯B=0.965 with total and chirp masses of m¯T,B=1670M⊙ and m¯c,M=642M⊙, respectively. We find that cluster puffing up and evaporation leads to bubbles of these PBHs of order 1 kpc containing at present times about 36% of objects and mass, with one-hundred pc-sized cores. We also find that these PBH sub-haloes are distributed in wider PBH haloes of order hundreds of kpc, containing about 63% of objects and mass, coinciding with the sizes of galactic halos. We find at last high rates of close encounters of massive Black Holes (M∼1000M⊙), with ΓS=(1.2+5.9−0.9)×107yr−1Gpc−3 and mergers with ΓM=1337±41yr−1Gpc−3.

scholarly journals Formation of Massive Black Holes in Dense Star Clusters. I. Mass Segregation and Core Collapse

2004 ◽  
Vol 604 (2) ◽  
pp. 632-652 ◽  
Author(s):  
M. Atakan Gurkan ◽  
Marc Freitag ◽  
Frederic A. Rasio
Keyword(s):  
Black Holes ◽  
Star Clusters ◽  
Core Collapse ◽  
Massive Black Holes ◽  
Mass Segregation

scholarly journals Planetary systems in a star cluster II: intermediate-mass black holes and planetary systems

2020 ◽  
Vol 497 (3) ◽  
pp. 3623-3637
Author(s):  
Francesco Flammini Dotti ◽  
M B N Kouwenhoven ◽  
Qi Shu ◽  
Wei Hao ◽  
Rainer Spurzem
Keyword(s):  
Black Holes ◽  
Star Clusters ◽  
Planetary Systems ◽  
Dynamical Evolution ◽  
Star Cluster ◽  
High Mass ◽  
Intermediate Mass ◽  
Massive Black Holes ◽  
Mass Segregation ◽  
Intermediate Mass Black Holes

ABSTRACT Most stars form in dense stellar environments. It is speculated that some dense star clusters may host intermediate-mass black holes (IMBHs), which may have formed from runaway collisions between high-mass stars, or from the mergers of less massive black holes. Here, we numerically explore the evolution of populations of planets in star clusters with an IMBH. We study the dynamical evolution of single-planet systems and free-floating planets, over a period of 100 Myr, in star clusters without an IMBH, and in clusters with a central IMBH of mass $100\, \mathrm{M}_\odot$ or $200\, \mathrm{M}_\odot$. In the central region ($r\lesssim 0.2$ pc), the IMBH’s tidal influence on planetary systems is typically 10 times stronger than the average neighbour star. For a star cluster with a $200\, \mathrm{M}_\odot$ IMBH, the region in which the IMBH’s influence is stronger within the virial radius (∼1 pc). The IMBH quenches mass segregation, and the stars in the core tend to move towards intermediate regions. The ejection rate of both stars and planets is higher when an IMBH is present. The rate at which planets are expelled from their host star rate is higher for clusters with higher IMBH masses, for t < 0.5trh, while remains mostly constant while the star cluster fills its Roche lobe, similar to a star cluster without an IMBH. The disruption rate of planetary systems is higher in initially denser clusters, and for wider planetary orbits, but this rate is substantially enhanced by the presence of a central IMBH.

Gravitational wave sources containing massive black holes

2003 ◽  
Vol 32 (7) ◽  
pp. 1243-1246 ◽  
Author(s):  
Peter L. Bender ◽  
Dieter Hils
Keyword(s):  
Black Holes ◽  
Gravitational Wave ◽  
Massive Black Holes

scholarly journals Dynamics of galactic nuclei: mass segregation and collisions

2007 ◽  
Vol 3 (S245) ◽  
pp. 211-214 ◽  
Author(s):  
Marc Freitag ◽  
James E. Dale ◽  
Ross P. Church ◽  
Melvyn B. Davies
Keyword(s):  
Black Holes ◽  
Galactic Nuclei ◽  
Stellar Mass ◽  
Galactic Centre ◽  
Massive Black Holes ◽  
Giant Stars ◽  
Mass Segregation

AbstractMassive black holes (MBHs) with a mass below ~ 107 M⊙ are likely to reside at the centre of dense stellar nuclei shaped by 2-body relaxation, close interactions with the MBH and direct collisions. In this contribution, we stress the role of mass segregation of stellar-mass black holes into the innermost tenths of a parsec and point to the importance of hydrodynamical collisions between stars. At the Galactic centre, collisions must affect giant stars and some of the S-stars.

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